//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31769 SUBJECT: GRB 220319A: Swift detection of a burst DATE: 22/03/19 18:07:27 GMT FROM: Kim Page at U.of Leicester K. L. Page (U Leicester), S. D. Barthelmy (GSFC), J.D. Gropp (PSU), J. A. Kennea (PSU), A. Y. Lien (U Tampa), D. M. Palmer (LANL) and T. M. Parsotan (GSFC/UMBC/CRESSTII) report on behalf of the Neil Gehrels Swift Observatory Team: At 17:40:33 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 220319A (trigger=1098132). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 218.207, +61.289 which is RA(J2000) = 14h 32m 50s Dec(J2000) = +61d 17' 20" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 10 sec. The peak count rate was ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 17:42:14.5 UT, 101.2 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 218.22471, 61.29389 which is equivalent to: RA(J2000) = 14h 32m 53.93s Dec(J2000) = +61d 17' 38.0" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 35 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. No spectrum from the promptly downlinked event data is yet available to determine the column density. UVOT took a finding chart exposure of 250 seconds with the U filter starting 317 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18.0 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.010. Burst Advocate for this burst is K. L. Page (kimlpage1978 AT gmail.com). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31770 SUBJECT: GRB 220319A: MASTER Global Robotic Net optical observations DATE: 22/03/19 18:09:16 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, A.Kuznetsov, O.Gress,E.Gorbovskoy, N.Tyurina, P.Balanutsa, K.Zhirkov, A.Chasovnikov, D.Vlasenko, G.Antipov, V.Senik, D.Kuvshinov, V.Topolev, Ya.Kechin, Yu.Tselik (Lomonosov Moscow State University, SAI, Physics Department), C.Francile, R. Podesta, C.Lopez, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA), D.A.H.Buckley (SAAO), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory), N.M.Budnev (ISU,API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational State University) MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the SWIFT BAT GRB 220319A (GRB220319.74, trigger No 1098132, 14h 32m 49.68s , +61d 17m 20.4s, R=0.05 Page et al. GCN 31769 https://gcn.gsfc.nasa.gov/other/1098132.swift ) errorbox 38 sec after notice time (62 sec after trigger time) at 2022-03-19 17:41:35 UT, with upper limit up to 15.6 mag . The observations began at zenith distance = 57 deg. The sun altitude is -19.9 deg. The galactic latitude b = 52 deg., longitude l = 103 deg. Real time updated cover map and OT, that can be discovered,will be available here: https://master.sai.msu.ru/site/master2/observ.php?id=1915275 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 67 | MASTER-Tavrida | P\ | 10 | 14.9 | 102 | MASTER-Tavrida | P\ | 20 | 15.6 | 142 | MASTER-Tavrida | P\ | 20 | 15.4 | The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31771 SUBJECT: GRB 220319A: Enhanced Swift-XRT position DATE: 22/03/20 07:19:20 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1697 s of XRT Photon Counting mode data and 2 UVOT images for GRB 220319A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 218.22421, +61.29496 which is equivalent to: RA (J2000): 14h 32m 53.81s Dec (J2000): +61d 17' 41.9" with an uncertainty of 2.2 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31772 SUBJECT: GRB 220319A: Swift-XRT refined Analysis DATE: 22/03/20 07:30:51 GMT FROM: Phil Evans at U of Leicester J. D. Gropp (PSU), J.P. Osborne (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto) and K.L. Page report on behalf of the Swift-XRT team: We have analysed 6.4 ks of XRT data for GRB 220319A (Page et al. GCN Circ. 31769), from 108 s to 36.4 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 31771). The light curve can be modelled with a power-law decay with a decay index of alpha=0.86 (+0.08, -0.07). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.2 (+0.5, -0.4). The best-fitting absorption column is 2.2 (+1.5, -1.2) x 10^21 cm^-2, in excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (4.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.2 (+1.5, -1.2) x 10^21 cm^-2 Galactic foreground: 1.5 x 10^20 cm^-2 Excess significance: 2.8 sigma Photon index: 2.2 (+0.5, -0.4) If the light curve continues to decay with a power-law decay index of 0.86, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.6 x 10^-14 (1.0 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01098132. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31773 SUBJECT: GRB 220319A: Mondy optical uper limit DATE: 22/03/20 09:57:51 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI, HSE), A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov (HSE) report on behalf of GRB IKI FuN: We observed the field of GRB 220319A (Page et al., GCN 31769) with AZT-33 telescope of Mondy observatory starting on Mar. 19 (UT) 18:25:41. We do not detect any optical counterpart within the Swift/XRT error box (Page et al., GCN 31769; Goad et al., GCN 31771). Preliminary photometry of the field is following Date UT start t-T0 Filter Exp. OT Err UL(3sigma) 2022-03-19 18:25:41 0.04523 R 40*60 n/d n/d 21.7 The photometry is based on the nearby SDSS-DR12 stars R (Lupton transformations) R.A. Dec R 14:33:05.13264 +61:18:55.9584 16.1498 14:32:35.99328 +61:17:16.0764 16.5417 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31774 SUBJECT: GRB 220319A: LCO Optical Upper Limit DATE: 22/03/20 10:22:27 GMT FROM: Robert Strausbaugh at U. of the Virgin Islands R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration: We observed Swift GRB 220319A (Page et al., GCN 31769) with the LCO 1-m Sinistro instrument at the Teide Observatory, Tenerife site, on March 19, from 23:48 to March 20, 00:15 UT (corresponding to 5.68 to 6.13 hours from the GRB trigger time) with the Bessel R and I filters. We performed a series of 3x300s exposures in I and R bands. We do not detect an optical counterpart within the XRT enhanced error region (Goad et al., GCN 31771) in either band, consistent with the non-detection from Mondy (Belkin et. al, GCN 31773). The following upper limits are calculated using the USNO-B.1 catalog as reference: R>21.44 I>20.47 These magnitudes are not corrected for galactic extinction. R.S. is funded by NSF AST grant #1831682 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31775 SUBJECT: GRB220319A: Optical observations from NOT DATE: 22/03/20 13:47:37 GMT FROM: Antonio de Ugarte Postigo at OCA A. de Ugarte Postigo (OCA) and R. Clavero Jimenez (NOT) report on behalf of a larger collaboration: We observed the field of GRB220319A (Page et al. GCN31769) with the 2.5m Nordic Optical Telescope equipped with AlFOSC. Observations consisted of 3x300s in r and 5x200s in z. Due to variable weather conditions, the observation was attempted twice, between 22:12 and 22:47 UT and between 00:10-00:48 UT (starting 4.53 and 6.49 hr after the burst). We also note the high background due to the illumination from the almost full Moon. The first attempt had a seeing of 1.5“ in r and 1.3“ in z and was affected by some dome vignetting due to the low elevation. The second observation had better conditions with 1.2“ seeing in r and 1.1“ in z. In a preliminary reduction, we do not detect any new source within or near the refined XRT position (Goad et al. GCN 31771) in any of the images. We estimate a 3-sigma limit of z > 21.5 mag in the first epoch and > 22.5 mag in the second epoch. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31776 SUBJECT: GRB 220319A: MITSuME Akeno optical upper limits DATE: 22/03/20 16:06:24 GMT FROM: Ryohei Hosokawa at Tokyo Institute of Technology R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, N. Ito, Y. Takamatsu, R. Noto, S. Sato, M. Takaku, R. Yamaguchi, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 220319A (K. L. Page et al. GCN Circular #31769, V.Lipunov et al. GCN Circular #31770, M.R. Goad et al. GCN Circular #31771, J. D. Gropp et al. GCN Circular #31772, S. Belkin et al. GCN Circular #31773, R. Strausbaugh et al. GCN Circular #31774, A. de Ugarte Postigo et al. GCN Circular #31775) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno. The observation with a series of 10 sec exposures started at 2022-03-19 17:41:30 UT (56.7 seconds after Swift BAT trigger). We stacked the images with good conditions. We did not detect any sources within the XRT error region (M.R. Goad et al. GCN Circular #31771). We obtained the 5-sigma limits of the stacked images as follows. T0+[sec] | MID-UT | T-EXP[sec] | 5-sigma limits ------------------------------------------------------------- 101 | 2022-03-19 17:42:14 | 50 | g'>17.0, Rc>16.8, Ic>16.5 762 | 2022-03-19 17:53:16 | 560 | g'>18.5, Rc>18.3, Ic>17.9 4925 | 2022-03-19 19:02:38 | 5520 | g'>19.8, Rc>19.9, Ic>19.6 ------------------------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31781 SUBJECT: GRB 220319A: Swift-BAT refined analysis DATE: 22/03/22 15:40:46 GMT FROM: Sibasish Laha at GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 220319A (trigger #1098132) (Page et al., GCN Circ. 31769). The BAT ground-calculated position is RA, Dec = 218.139, 61.291 deg which is RA(J2000) = 14h 32m 33.4s Dec(J2000) = +61d 17' 26.6" with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 43%. The BAT light curve showed a single-peaked structure with a duration of about 10 sec. T90 (15-350 keV) is 6.44 +- 1.54 sec (estimated error including systematics). The time-averaged spectrum from T-0.36 to T+6.56 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.15 +- 0.28. The fluence in the 15-150 keV band is 2.3 +- 0.4 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T-0.24 sec in the 15-150 keV band is 1.5 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/1098132/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 31785 SUBJECT: GRB 220319A: GRANDMA observations DATE: 22/03/24 14:29:52 GMT FROM: Marie Anne Bizouard at ARTEMIS/CNRS M. Bizouard (OCA/Artemis), P-A. Duverne (IJCLAB), A. Iskandar (XAO), D. Datashvili (AbAO), M. Blazek (FZU), D. Turpin (CEA), T. Midavaine (KNC) S. Antier (OCA/Artemis), I. Tosta eMelo (INFN-LNS), X. F. Wang (TSU/BJP), J. Zhu (BJP), X. Song (BJP), S. Karpov (FZU), A. Kann (IAA-CSIC), D. Marchais (KNC), A. Popowicz (KNC), A. Oksanen (KNC), M. Serrau (KNC), M. Freeberg (KNC),  A. Klotz (IRAP-OMP), R. Kneip (KNC), E. Broens (KNC), O. Aguerre (KNC), report  on behalf of the GRANDMA collaboration: The GRANDMA telescope network responded to the alert of GRB 220319A (Page et al. GCN 31769). The first observations started 14 min after the BAT trigger time. No new object was detected within the XRT enhanced error region (Goad et al. GCN 31771). The observations were affected by the nearby full Moon and in some cases also by Sahara dust. In the following table we report the preliminary photometry of our observations. Upper limits are reported at the 3-sigma limit, in the AB system. T-T0 (hr)| MJD    | Observatory| Filter| Upp.Mag. ____________________________________________________ 0.23 |59657.746539| KNC-HAN    |  Lum      | 18.6 0.94 |59657.775880| KNC-HAN    |  Lum      | 18.7 1.38 |59657.794039| KNC-TJML   |  Clear    | 15.7 2.79 |59657.852604| KNC-T-BRO  |  Clear    | 18.6 2.89 |59657.856921| KNC-K26    |  Lumen    | 18.2 4.01 |59657.903715| KNC-T-CAT  |  Blue     | 19.4 4.01 |59657.903715| KNC-T-CAT  |  Green    | 19.5 4.01 |59657.903715| KNC-T-CAT  |  Red      | 18.2 5.47 |59657.964502| KNC-TJMS-PS|  Lumen    | 20.0 5.62 |59657.970540| ALi-50     |  Clear    | 20.1 7.22 |59658.037350| KNC-T-AGU  |  Lum      | 18.8 10.85|59658.188623| C11FREE    |  Rc       | 18.7 Most of these observations were performed in the context of the Kilonova-Catcher programme (KNC), a professional-amateur collaboration within the GRANDMA project, and in some cases using non-standard filters. The KNC images have been processed using the MUPHOTEN pipeline (Duverne et al. 2021) and photometry was performed using field stars from the PanSTARRS catalogue as reference. GRANDMA is a worldwide coordinated telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).